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Table 2.

Molecular gas properties of the Seyfert 2 galaxies.

Name Spectral line ICO[2–1] SCO[2–1] rms WCO αCO log(MH2) fap Ref.
K km s−1 Jy km s−1 mK km s−1 log(K km s−1 pc2) M pc−2 (K km s−1)−1 log(M)
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)
CGCG 381-051 CO(2–1) 3.4 ± 0.3 127 ± 15 0.54 187 ± 3 9.24 ± 0.06 4.30 ± 1.01 9.88 ± 0.10 1.31 ± 0.05 (a)
ESO 033-G002 CO(2–1) 0.67 ± 0.07 25 ± 3 0.32 161 ± 6 8.14 ± 0.06 2.88 ± 1.00 8.60 ± 0.15 1.54 ± 0.07 (a)
IC 5063 CO(2–1) 3 ± 0.29 111 ± 13.96 0.63 385 ± 5 8.84 ± 0.07 4.57 ± 1.05 9.50 ± 0.10 4.40 ± 0.13 (a)
IRAS F01475-0740 CO(2–1) 2.23 ± 0.18 82.65 ± 9.49 0.58 87.8 ± 1.1 8.49 ± 0.06 4.17 ± 1.06 9.11 ± 0.11 1.11 ± 0.01 (a)
IRAS F04385-0828 CO(2–1) 1.77 ± 0.14 65.35 ± 7.49 0.25 142 ± 1.6 8.32 ± 0.06 2.69 ± 0.99 8.75 ± 0.16 1.27 ± 0.07 (a)
IRAS F15480-0344 CO(2–1) 1.1 ± 0.12 40.7 ± 5.41 0.5 150 ± 5 8.67 ± 0.08 4.07 ± 1.13 9.28 ± 0.12 1.13 ± 0.04 (a)
MCG-03-34-064 CO(2–1) 2.56 ± 0.26 94.66 ± 12.34 0.75 334 ± 11 8.75 ± 0.06 1.55 ± 0.75 8.94 ± 0.21 1.97 ± 0.15 (a)
MCG-03-58-007 CO(2–1) 6.57 ± 0.54 243.14 ± 28.16 0.73 319 ± 4 9.58 ± 0.06 1.95 ± 0.81 9.87 ± 0.18 1.41 ± 0.02 (a)
MCG+00-29-023 CO(2–1) 15.45 ± 1.21 571.82 ± 64.42 0.5 361.2 ± 1.1 9.75 ± 0.05 2.51 ± 0.69 10.15 ± 0.12 1.42 ± 0.07 (a)
Mrk 0273 CO(1–0) 9.95 ± 0.06 1.45 ± 0.60 10.11 ± 0.18 1.38 ± 0.03 (b)
Mrk 0463 CO(2–1) 1.74 ± 0.18 64.39 ± 8.43 0.53 228 ± 7 9.47 ± 0.06 5.25 ± 0.97 10.19 ± 0.08 1.62 ± 0.18 (a)
Mrk 0897 CO(2–1) 3.75 ± 0.31 138.87 ± 16.2 0.6 216 ± 3 9.14 ± 0.07 1.86 ± 0.82 9.41 ± 0.19 1.31 ± 0.01 (a)
NGC 0034 CO(1–0) 9.51 ± 0.06 1.62 ± 0.75 9.72 ± 0.20 1.29 ± 0.04 (c)
NGC 0424 CO(2–1) 0.9 ± 0.08 33.4 ± 4.02 0.17 258 ± 6 8.07 ± 0.06 3.39 ± 1.09 8.6 ± 0.14 2.31 ± 0.04 (a)
NGC 0513 CO(1–0) 9.01 ± 0.08 3.16 ± 1.24 9.51 ± 0.17 1.06 ± 0.05 (d)
NGC 1125 CO(2–1) 2.1 ± 0.17 77.84 ± 8.87 0.21 228 ± 2 8.33 ± 0.06 3.16 ± 1.09 8.83 ± 0.15 2.12 ± 0.09 (a)
NGC 1320 CO(2–1) 2.61 ± 0.23 96.58 ± 11.69 0.43 338 ± 8 8.34 ± 0.10 3.31 ± 1.07 8.86 ± 0.14 2.60 ± 0.20 (a)
NGC 2992 CO(2–1) 12.99 ± 1.02 480.52 ± 54.25 0.52 492 ± 3 9.14 ± 0.06 2.04 ± 0.71 9.45 ± 0.15 4.41 ± 0.01 (a)
NGC 3079 CO(1–0) 9.79 ± 0.05 0.59 ± 0.33 9.56 ± 0.24 7.18 ± 0.3 (d)
NGC 4388 CO(2–1) 9.81 ± 0.06 3.02 ± 0.56 10.29 ± 0.08 15.87 ± 0.02 (e)
NGC 4602 CO(2–1) 8.96 ± 0.74 331.56 ± 38.28 1.38 148.1 ± 1.9 8.70 ± 0.06 3.39 ± 0.86 9.23 ± 0.11 1.92 ± 0.03 (a)
NGC 5135 CO(1–0) 10.24 ± 0.04 0.69 ± 0.33 10.08 ± 0.21 5.10 ± 0.06 (b)
NGC 5256 CO(1–0) 10.16 ± 0.04 1.70 ± 0.51 10.39 ± 0.13 2.20 ± 0.20 (b)
NGC 5347 CO(1–0) 8.39 ± 0.06 2.69 ± 0.93 8.82 ± 0.15 1.41 ± 0.11 (d)
NGC 5506 CO(2–1) 6.68 ± 0.54 246.99 ± 28.37 0.7 327 ± 4 8.65 ± 0.06 3.24 ± 0.89 9.16 ± 0.12 4.31 ± 0.01 (a)
NGC 5953 CO(2–1) 20.88 ± 1.63 772.68 ± 87.02 0.72 204.3 ± 0.7 8.91 ± 0.10 2.24 ± 0.62 9.26 ± 0.12 2.20 ± 0.04 (a)
NGC 5995 CO(2–1) 9.82 ± 0.78 363.27 ± 41.13 0.5 420 ± 3 9.61 ± 0.06 1.78 ± 0.74 9.86 ± 0.18 1.61 ± 0.07 (a)
NGC 6890 CO(2–1) 9.45 ± 0.78 349.82 ± 40.38 1.21 237 ± 3 8.78 ± 0.06 1.78 ± 0.70 9.03 ± 0.17 2.38 ± 0.03 (a)
NGC 7130 CO(1–0) 9.77 ± 0.04 2.19 ± 0.71 10.11 ± 0.14 1.58 ± 0.08 (c)
NGC 7496 CO(2–1) 13.52 ± 1.06 500.22 ± 56.42 1.23 89.4 ± 0.4 9.00 ± 0.06 3.31 ± 0.76 9.52 ± 0.10 6.10 ± 0.30 (a)
NGC 7674 CO(2–1) 11.44 ± 0.9 423.34 ± 47.9 0.79 194.8 ± 1.2 9.83 ± 0.06 1.86 ± 0.64 10.10 ± 0.15 1.73 ± 0.18 (a)
TOLOLO 1238-364 CO(2–1) 7.58 ± 0.61 280.62 ± 32.08 0.93 151.5 ± 1.9 8.84 ± 0.8 2.75 ± 0.95 9.28 ± 0.15 1.90 ± 0.03 (a)
UGC 05101 CO(1–0) 10.10 ± 0.06 1.15 ± 0.56 10.16 ± 0.21 2.20 ± 0.30 (b)

Notes. Column descriptions: (1) source name; (2) CO transition considered; (3) CO integrated line intensity in units of K km s−1 from the new APEX observations; (4) CO flux in units of Jy km s−1; (5) RMS of the CO line in units of mK; (6) CO line width in units of km s−1; (7) logarithm of the aperture-corrected in K km s−1 pc2; (8) logarithm of the aperture-corrected molecular gas mass (MH2) in units of M; (9) adopted aperture correction factor with the associated error (see Sect. 3.1.3); and (10) references to the CO spectroscopy: (a) this paper, (b) Papadopoulos et al. (2012), (c) Albrecht et al. (2007), (d) Maiolino et al. (1997), and (e) Rosario et al. (2018).

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